However, there are a few black holes which have intrinsically much
lower columns which have been observed with CCD detectors, namely XTE
J1118+480: \(N_H\sim 1.1\times 10^{20}\)  cm\(^{-2}\) , XTE J1817-330:
\(1.1\times 10^{21}\)  cm\(^{-2}\)  and SWIFT1753.5-0127: \(2-3\times 10^{21}\)  cm\(^{-2}\)  [1]}. XTE J1118+480 has only
snapshot spectra available ([2]}; [3]};
[4]}; 2003), but both SWIFT1753.5-0127 and XTE
J1817-330 were well sampled throughout their outbursts by the Swift
satellite. However, XTE J1817-330 is a long period system, so spends
most of its time in the disc dominated state, with only two, rather
faint, LHS spectra at the end of its outburst. Thus the short period
LHS outburst of SWIFT1753.5-0127 is the best candidate to study the
disc evolution in the LHS. Here we analyse these data with
sophisticated models to describe the behaviour of the X-ray irradiated
disc (GDP08; [5]}, hereafter GDP09) to constrain its inner radius as the outburst declines.
